Formation of Accretion Disks in Close-Binary Systems with Magnetic Fields

Abstract

We have developed a three-dimensional numerical model and applied it to simulate plasma flows in semi-detached binary systems whose accretor possesses a strong intrinsic magnetic field. The model is based on the assumption that the plasma dynamics are determined by the slow mean flow, which forms a backdrop for the rapid propagation of MHD waves. The equations describing the slow motion of matter were obtained by averaging over rapidly propagating pulsations. The numerical model includes the diffusion of magnetic field by current dissipation in turbulent vortices, magnetic buoyancy, and wave MHD turbulence. A modified three-dimensional, parallel, numerical code was used to simulate the flow structure in close binary systems with various accretor magnetic fields, from $10^5$ to $10^8$ G. The conditions for the formation of the accretion disk and the criteria distinguishing the two types of flow corresponding to intermediate polars and polars are discussed.

20 pages, 12 figures, Submitted in Astronomy Reports, 2010, 54, No. 12

References in corpus (4)

• The spin periods and magnetic moments of white dwarfs in magnetic cataclysmic variables
• The Accretion Flows and Evolution of Magnetic Cataclysmic Variables
• The Spin Period of EX Hydrae
• On the mass transfer in AE Aquarii

Cited by in corpus (7)

• 3D MHD Simulations of Accretion onto Stars with Tilted Magnetic and Rotational Axes
• Full 3-D MHD calculations of accretion flow Structure in magnetic cataclysmic variable stars with strong and complex magnetic fields
• Colliding Winds in Low-Mass Binary Star Systems: wind interactions and implications for habitable planets
• Features of the Matter Flows in the Peculiar Cataclysmic Variable AE Aquarii
• A Numerical Model for Accretion in Intermediate Polars with Dipolar Magnetic Fields
• Features of the Accretion in the EX Hydrae System: Results of Numerical Simulation
• Features of the Flow Structure in the Vicinity of the Inner Lagrangian Point in Polars